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From figure 8 we observe that much of the data is clustered in the bottom right corner of the figure. This is because of a geometric effect, where the area in an annulus with $ r_{p}$-lower = 50 & $ r_{p}$-higher is much greater than for $ r_{p}$-lower = 0 & $ r_{p}$-higher = 50. We also note that the pair velocity offset seems to increase slightly with a increase in the projected separation. Since the luminosity of FR-I galaxies falls below a threshold luminosity$ 2 \times 10^{25} W Hz^{-1}sr^{−1}$ , we observe from Figure 12 that our sample data can be categorized as FR-I. We have also stated that most FR-II sources are found at redshift ∼ 0.2 − 0.3.   From Figure 9 we observe as the pair velocity decreases -because of the closer interaction of the quasar pairs- the redshift (and thus the luminosity) increases. We see this the data points This is because accretion onto SMBHs releases energy that drives outflows.  From Figure 11, we observe that as the separation between quasar pairs decreases the accretion rate, thus the luminosity of the core increases.